Solar Terrestrial Activity Report

Activity chart

Last major update issued on September 8, 2017 at 04:50 UT.

Charts (* = updated daily) Data and archive
  Solar wind (*) Solar and geomagnetic data - last month (*)
  Electron fluence (*) Archived daily reports and monthly data since 2003.01 (August 2, 2017)
Solar cycle Solar cycles 23-24 (September 1, 2017) Historical solar and geomagnetic data charts 1954-2006 (April 5, 2007)
  Cycle 24 progress (September 1, 2017) Noon SDO sunspot count 1K / 4K (*)
  Solar cycles 1-24 (July 17, 2015) POES auroral activity level October 2009 - December 2012]
  Comparison of cycles 21, 22, 23 and 24 (September 1, 2017) 3rd SSN Workshop, Tucson, 2013
  Comparison of cycles 12, 13, 14, 16 and 24 (September 1, 2017) 4th SSN Workshop, Locarno, 2014
  Solar polar fields vs. solar cycles (July 16, 2017)  

Recent activity

The geomagnetic field was quiet to severe storm on September 7. Solar wind speed at SOHO ranged between 446 and 806 km/s. Earth received a direct hit from the CME observed on September 6 after the X9 flare. A strong solar wind shock was observed at 22:38 at SOHO, which makes the transit time for this CME only 35 hours. The geomagnetic field was initially at severe to very severe storm levels.

Solar flux at 20h UTC on 2.8 GHz was 128.5 (increasing 58.7 over the previous solar rotation). The average 90 day 10.7 flux at 1 AU was 82.1. The Potsdam WDC planetary A index was 34 (STAR Ap - based on the mean of three hour interval ap indices: 34.3). Three hour interval K indices: 34333247 (planetary), 24454326 (Boulder)

The background x-ray flux is at the class B8 level.

At the time of counting spots (see image time), spots were observed in 6 active regions using 2K resolution (SN: 200) and in 6 active regions using 1K resolution (SN: 132) SDO images on the visible solar disk.

Region 12673 [S09W56] became slightly less complex as opposite polarity umbrae within the same penumbra showed increased separation and a shorter inversion line. Further X class events are possible until the region rotates out of view. There is a chance for a strong proton flare as the region approaches the southwest limb.
Region 12674 [N13W42] decayed slowly and quietly.
Region 12677 [N17E11] was quiet and stable.
Region 12678 [N10E20] was quiet and stable.
New region 12679 [N15W26] emerged on September 5 and was numbered by SWPC 2 days later.

Spotted regions not numbered (or interpreted differently) by SWPC:
S5791 [S09W12] decayed slowly and quietly.

C2+ flares:

Magnitude Peak time (UT) Location AR Recorded by Comment
M2.4/1F 05:02 S07W45 12673 GOES15  
C8.2/1F 06:28 S08W46 12673 GOES15  
C2.3 09:20   12673 GOES13  
M1.4/1N 09:54 S08W46 12673 GOES15  
M7.3 10:15   12673 GOES15  
C3.0 12:14 S08W48 12673 GOES15  
X1.3/2B 14:36 S08W51 12673 GOES15  
C5.2 18:28   12673 GOES15  
C4.5 18:44   12673 GOES15  
C2.5 20:57   12673 GOES15  
C5.4 21:37   12673 GOES15  
C2.7 23:00   12673 GOES15  

Coronal mass ejections (CMEs)

September 6: A large and fast CME was observed after the X9 event in AR 12673. This CME reached Earth late on September 7 with a transit time of 35 hours.
September 5,7
: No obviously Earth directed CMEs were observed in available LASCO imagery.

Coronal holes

[Coronal hole history (since October 2002)]
[Compare today's report to the situation one solar rotation ago: 28 days ago 27 days ago 26 days ago]

A recurrent southern hemisphere coronal hole (CH823) was in an Earth facing position on September 4-5. CH823 is not expected to produce any terrestrial effects due to the ongoing CME related disturbances. A recurrent northern hemisphere coronal hole (CH824) will likely rotate across the central meridian on September 10-12.

Propagation

Long distance low and medium frequency (below 2 MHz) propagation along paths north of due west over upper middle latitudes is very poor. Propagation on long distance northeast-southwest paths is very poor.

Forecast

The geomagnetic field is expected to be unsettled to major storm on September 7-9 due to CME effects.

Coronal holes (1) Coronal mass ejection (2) M and X class flares (3)
     

1) Effects from a coronal hole could reach Earth within the next 5 days. When the high speed stream has arrived the color changes to green.
2) Effects from a CME are likely to be observed at Earth within 96 hours.
3) There is a possibility of either M or X class flares within the next 48 hours.

Green: 0-30% probability, Yellow: 30-70% probability, Red: 70-100% probability.

Active solar regions


(Click on image for 2K resolution). 4K resolution. Compare to the previous day's image.
0.5K image

When available the active region map has a coronal hole polarity overlay where red (pink) is negative and blue is positive.

Data for all numbered solar regions according to the Solar Region Summary provided by NOAA/SWPC. Comments are my own, as is the STAR spot count (spots observed at or inside a few hours before midnight) and data for regions not numbered by SWPC or where SWPC has observed no spots. SWPC active region numbers in the table below and in the active region map above are the historic SWPC/USAF numbers.

Active region Date numbered
detected
Spot count Location at midnight Area Classification SDO / HMI 4K continuum
image with magnetic polarity overlays
Comment
SWPC Magnetic
(SDO)
SWPC STAR Current Previous
2K 1K
12673 2017.08.28
2017.08.29
21 51 30 S09W58 1000 EKC DKC location: S09W56

beta-gamma-delta

12674 2017.08.28
2017.08.29
13 35 17 N14W41 0600 FKO FKO

 

12677 2017.09.02
2017.09.03
3 20 8 N17E12 0010 BXO DRI area: 0035
S5788 2017.09.02       S10W09            
12678 2017.09.04
2017.09.05
3 13 10 N11E18 0040 HAX CRI  
12679 2017.09.05
2017.09.07
4 19 6 N14W27 0010 BXO CRO area: 0040
S5791 2017.09.06   2 1 S09W12 0003   AXX  
Total spot count: 44 140 72  
Sunspot number: 94 200 132  (total spot count + 10 * number of spotted regions)
Weighted SN: 69 169 101  (Sum of total spot count + classification weighting for each AR. Classification weighting: X=0, R=3, A/S=5, H/K=10)
Relative sunspot number (Wolf number): 103 110 106 k * (sunspot number)
As of May 7, 2016: k = 1.1 for SWPC, k = 0.55 for MSN 2K, k = 0.80 for MSN 1K (MSN=Magnetic Sunspot Number)

Monthly solar cycle data

Month Average solar flux International sunspot number
(WDC-SILSO) (4)
Smoothed sunspot number (4) Average ap
(3)
Measured 1 AU
2014.02 170.3
(cycle peak)
166.3 146.1 (cycle peak) 110.5 (+1.2) 10.70
2014.04 143.9 144.8 112.5 116.4 (+2.1) (solar max) 7.88
2016.04 93.3 94.0 38.0 47.8 (-2.7) 9.03
2016.05 93.0 95.3 52.1 44.9 (-2.9) 11.65
2016.06 81.9 84.5 20.9 41.6 (-3.3) 8.44
2016.07 86.0 88.9 32.5 38.6 (-3.0) 9.43
2016.08 85.0 87.1 50.7 36.0 (-2.6) 9.61
2016.09 87.7 88.7 44.7 33.3 (-2.7) 14.54
2016.10 86.1 85.6 33.6 31.4 (-1.9) 15.33
2016.11 78.6 76.9 21.4 29.9 (-1.5) 9.11
2016.12 75.1 72.8 18.9 28.5 (-1.4) 9.34
2017.01 77.3 74.9 25.8 27.9 (-0.6) 9.45
2017.02 76.8 75.0 26.1 26.6 (-1.3) 9.58
2017.03 74.6 73.9 17.7 (25.0 projected, -1.6) 14.20
2017.04 80.3 80.8 32.6 (23.4 projected, -1.6) 11.70
2017.05 73.6 75.2 18.8 (22.3 projected, -1.1) 8.09
2017.06 74.7 77.1 19.4 (21.3 projected, -1.0) 6.08
2017.07 77.4 79.9 18.3 (20.2 projected, -1.1) 8.97
2017.08 77.9 79.8 33.1 (18.7 projected, -1.5) 10.1
2017.09 (117.7)   20.8 (2A) / 92.3 (2B) / 49.1 (2C) (17.5 projected, -1.2) (15.4)

1) Running average based on the daily 20:00 UTC observed solar flux value at 2800 MHz.
2A) Current impact on the monthly sunspot number based on the Boulder (NOAA/SWPC) sunspot number (accumulated daily sunspots / month days).
2B) Boulder SN current month average to date.
2C) STAR SDO 1K Wolf number 30 day average.
3) Running average based on the quicklook and definitive Potsdam WDC ap indices. Values in red are based on the definitive international GFZ Potsdam WDC ap indices.
4) Updated to new data set from WDC-SILSO on July 1, 2015

This report has been prepared by Jan Alvestad. It is based on the analysis of data from whatever sources are available at the time the report is prepared. All time references are to Universal Time. Comments and suggestions are always welcome.

SDO images are courtesy of NASA/SDO and the AIA, EVE, and HMI science teams.